adsabs/AstroCLIMB huggingface dataset:
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) sSFR as derived from the PAH 11.3 μm feature (Wu et al. 2009) and the calibration from Xie & Ho (2019) as a function of the bolometric luminosity as derived from the IR for all objects divided into Compton-thin (blue squares) and Compton-thick (red triangles). (b) Same as panel (a) but with the color coded objects and the fit of Compton-thin type 1 galaxies and all type 2 galaxies.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) BHAR as derived from the [O IV] 25.89 μm line luminosity and the calibration from Mordini et al. (2021), adopting the bolometric correction of Lusso et al. (2012) as a function of the black hole mass for all objects divided into Compton-thin (blue squares) and Compton-thick (red triangles). (b) Same as panel (a) but with the color coded objects and the fit of Compton-thin type 1 galaxies and all type 2 galaxies. Excluding the LINERs, an increasing trend of the BHAR as a function of the black hole mass is apparent in the data.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) SFR as derived from the sum of the [Ne III] 15.55 and [Ne II] 12.81 μm luminosities and the calibration of Mordini et al. (2021) with the correction for AGN from Zhuang et al. (2019) as a function of the BHAR as derived from the [O IV] 25.89 μm line luminosity and the calibration from Mordini et al. (2021), adopting the bolometric correction of Lusso et al. (2012) for all objects and only Compton-thin galaxies. Blue squares indicate Compton-thin objects, while red triangles are Compton-thick. The solid line shows the fit for all Compton-thin AGN, while the dashed line is the fit for all objects. (b) Same as panel (a) but with the color coded objects and the fit of Compton-thin type 1 galaxies and all type 2 galaxies. The value of the correlations is given in Table 7.
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (14–195) keV intrinsic flux as a function of the nuclear 12 μm flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (14–195) keV intrinsic luminosity vs. 12 μm luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) X-ray (2–10) keV intrinsic flux as a function of the nuclear 12 μm flux for all sources with reliable hard X-ray data and an optical spectroscopic classification. The blue squares indicate the Compton-thin AGN, while Compton-thick objects are denoted by red triangles. The solid line represents the linear regression fit with all objects, while the dashed line is the fit with only Compton-thin objects. (b) X-ray (2–10) keV intrinsic luminosity vs. 12 μm luminosity (both in logarithmic units of erg s−1).
Paper: The High-ionization IR Fine Structure Lines as Bolometric Indicators of the AGN Power: Study of the Complete 12 μm AGN Sample
Authors: Luigi Spinoglio, Juan Antonio Fernández-Ontiveros, Matthew A. Malkan
Figure caption: (a) SFR derived from the neon mid-IR fine structure lines as a function of the stellar mass of the galaxies. The galaxies are divided into Compton-thick and Compton-thin, and the given fits are indistinguishable. The dotted–dashed line represents the so-called main sequence for star-forming galaxies (Elbaz et al. 2011). (b) Same as panel (a) but with the color coded galaxy types.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: Spatially resolved [N II] BPT diagrams and WHAN diagrams for each galaxy. Left: SDSS 3-color image with composite, AGN, and star-forming classified spaxels in green, orange, and blue respectively, next to the [N II]/Hα vs. [O III]/Hβ diagram for each galaxy with the same coloring. The solid black line represents data from Kewley et al. (2001), and the dashed line is from Kauffmann et al. (2003a). Right: SDSS 3-color image with star-forming, weak AGN, strong AGN, and retired classified spaxels in teal, brown, pink, and red, respectively, alongside the WHAN diagram, W(Hα) vs. [N II]/Hα with classification boundaries from Cid Fernandes et al. (2011).
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: Total molecular gas and stellar masses for our cPSB galaxies and rPSB galaxies in purple and orange, respectively, with comparison samples plotted. The dotted and dashed lines show constant molecular gas fractions of 1% and 10%, respectively. The blue contours show star-forming galaxies from de los Reyes & Kennicutt (2019). In the left panel, the ALMaQUEST SF, GV, and SB samples are plotted in teal, green, and white pentagons, respectively, with molecular gas masses and SFRs summed within 1.5 R  e  of each galaxy. The error bar in the upper left shows typical uncertainties for the ALMaQUEST galaxies. In the right panel, two unresolved studies of PSB galaxies are shown, French et al. (2015), a sample of E+A galaxies in light green triangles, and Rowlands et al. (2015) in pink diamonds, a sample of PSB galaxies spanning a range of post-burst ages. Downward-pointing green triangles represent French et al. (2015) E+As with gas mass upper limits. ETGs from the ATLAS3D survey (Young et al. 2011) are plotted as dark red stars. We use the same α CO = 4.35M ⊙ (K km s−1 pc2)−1 for all samples plotted. Our PSB galaxies have a wide range of molecular gas fractions; while some of our PSB galaxies are very gas-rich, others have little molecular gas.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: Correlations between the log molecular gas fraction (﹩{M}_{{{\rm{H}}}_{2}}﹩/M *) of PSB regions and SFH parameters. cPSB galaxies are plotted in purple and rPSB galaxies in orange. Kendall’s τ correlation coefficient (including upper limits) and accompanying p-value are shown in the bottom right of each panel. We do not observe a significant correlation between any of the plotted quantities. Left: log molecular gas fraction vs. the time since the burst, approximately the time since the peak of the starburst. Center: log molecular gas fraction and the fraction of stellar mass formed in the recent starburst. Right: log molecular gas fraction and the fraction of stellar mass formed in the last Gyr.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: The Kennicutt–Schmidt relation between star formation surface density and molecular gas surface density for the PSB regions in our sample in purple for cPSB galaxies and orange for rPSB galaxies. We plot the ALMaQUEST SF, GV, and SB galaxies as blue, green, and white pentagons, respectively. The dashed line shows the measured relation from de los Reyes & Kennicutt (2019) with the estimated scatter shaded in gray.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: Histograms showing the Radon classifications for stellar velocity fields on the left and Hα velocity fields on the right. cPSB galaxies are plotted in purple, rPSB galaxies in orange, and ALMaQUEST star-forming galaxies in blue. Due to our small sample, we combine the inner bend, outer bend, and inner bend + outer bend classifications from Stark et al. (2018) into the symmetric bend category. In both panels, PSB galaxies show an excess of asymmetric velocity fields.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: The SFE (SFR/﹩{M}_{{{\rm{H}}}_{2}}﹩) and molecular gas fraction (﹩{M}_{{{\rm{H}}}_{2}}/{M}_{* }﹩) for PSB regions (cPSB galaxies in purple, and rPSB galaxies in orange) and the ALMaQUEST star-forming galaxies. The downward arrow shows an upper limit in SFR, and the diagonally pointing arrows show an upper limit in ﹩{M}_{{{\rm{H}}}_{2}}﹩ with constant SFR and M *.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: PCA classification boundaries in PC1 (D n 4000) and PC2 (excess Balmer absorption). The shaded regions show the boundaries for quiescent (red), SF (blue), GV (green), PSB (purple), and SB (yellow) classifications. The gray contours show the parent DR15 MaNGA sample, with levels corresponding to 1%, 5%, 30%, 50%, and 90% of the largest bin. The black and colored points show all spaxels from galaxies in the Chen et al. (2019) and PCA combined sample. The colored points are spaxels within those galaxies that are classified as PSB with the Chen et al. (2019) selection method, and are color coded according to their Hδ  A .
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: PCA classification results for 8939-3703. Left: the SDSS 3-color image, with a clear foreground star. Center: the excess Balmer absorption of each spaxel. Teal regions correspond to greater Balmer absorption, and to PSB regions. Right: the PCA classification from Rowlands et al. (2018), with PSB spaxels in purple, star-forming spaxels in blue, and starburst spaxels in teal. The green circle shows the MaNGA 2.″5 average seeing. This galaxy is clearly classified as a PSB.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: SFEs and molecular gas fractions computed with a varying α CO from Narayanan et al. (2012) for the PSB regions in our sample, with ﹩Z^{\prime} =2﹩. PSB regions of cPSB galaxies are plotted as circles, and PSB regions of rPSB galaxies are plotted as squares. These markers are colored by their computed α CO value. We also plot ALMaQUEST star-forming galaxies, with a Milky Way α CO of 4.35 M ⊙ (K km s−1 pc2)−1.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: Spectral index as a function of Galactic latitude averaged over 20″ segments of the NTFs. The error bars represent the standard deviation of the spectral index within each of these 20″ segments. The change in latitude from left to right in these panels roughly corresponds to tracing the filament lengths from the lower left to the upper right in the figures presented in Section 3.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: 10 GHz total-intensity distribution of SNTF3 (G359.69-0.14). This image has a beam size of 4.″6 × 1.″7 with an rms noise level of ∼20 μJy beam−1.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Temporal variation of the internal maser features. The size of the circle indicates the logarithm of the flux density of the maser spot (see the fourth subpanel for each maser feature as a legend). The color of the circle indicates the LSR velocity of the spot (see the third subpanel).
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Expansion of the BX Cam flow traced by H2O masers. The positional reference is Gaia EDR3 (red star). The black circle denotes the fitted ring of SiO masers in Section 3.3.3. The different colors of the maser spots indicate different observation epochs, which are astrometrically fixed using the method in Figure 8. An auxiliary dashed line indicates a possible trajectory of a maser feature from 2012 to 2022 at a constant-velocity vector, while the nearby lines in light gray show the position error of the back-extrapolated motion vectors. The lines of motion are drawn with the positions and proper motions of the maser features estimated in Table 2.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: The top view (left panel: R.A.–distance, XZ-plane) and the east-side view (right panel: distance–decl., ZY-plane) of the estimated positions and proper motions with respect to the outflow origin, using the method of Imai et al. (2000). The base of the arrow is pointed toward the position of the maser feature. The direction and length of the arrow represent the direction and magnitude of the proper motion, respectively. The red and blue arrows show the maser feature motions found in the EAVN (ESTEMA) and VERA observations (Matsuno et al. 2020), respectively.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: The registered maser flows from EAVN (ESTEMA) and VERA (Table 4 of Matsuno et al. 2020) observed at different pulsation circles. The registration is performed with Gaia EDR3. The numbers around the maser features are the three-dimensional velocities in km s−1.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Angular distance–LSR velocity diagram. The position of the star was used as the center of the SiO maser ring.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Same as Figure 9, but the different colors of the maser spots indicate different LSR velocities.
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Time evolution of the total (proton + electron) internal energy ﹩{{ \mathcal E }}^{\mathrm{th}}={{ \mathcal E }}_{{\rm{p}}}^{\mathrm{th}}+{{ \mathcal E }}_{{\rm{e}}}^{\mathrm{th}}﹩, the time-integrated total (proton + electron) pressure–strain rate ﹩-({\boldsymbol{P}}\cdot {\rm{\nabla }})\cdot {\boldsymbol{u}}=-({{\boldsymbol{P}}}_{{\rm{i}}}\cdot {\rm{\nabla }})\cdot {{\boldsymbol{u}}}_{{\rm{i}}}-({{\boldsymbol{P}}}_{{\rm{e}}}\cdot {\rm{\nabla }})\cdot {{\boldsymbol{u}}}_{{\rm{e}}}﹩, and the time-integrated ohmic dissipation rate  j  ·  E  from a fully kinetic, 2.5D particle-in-cell simulation using the code P3D (Zeiler et al. 2002). The time integration is performed from an initial time of 32.5 ω ci, and the difference in the internal energy from the initial time is shown. More details of the simulation can be found in the Appendix and in Parashar et al. (2018) and Adhikari et al. (2021).
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Comparison of the von Kármán decay rates and the inertial range flux derived from the Politano–Pouquet law for the MMS intervals. The computed rates were divided into nine bins and the averages in each bin are shown.
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Ratio of proton to electron heating rate vs. total (proton + electron) heating rate. For MMS results, −Π ij  D  ij  (averaged over each interval), identified as the heating rate (i.e., ﹩{Q}_{{\rm{s}}}=-{{\rm{\Pi }}}_{{ij}}^{({\rm{s}})}{D}_{{ij}}^{({\rm{s}})}﹩), is shown by red squares. The total and relative heating rates were accumulated into six bins, and the averages in these bins are shown here. Only intervals with positive ion and electron heating rate were considered. The points indicate that the relative heating of protons increases with the total heating rate (the solid line, with a slope of 1/3, is given for reference). The horizontal axis has been normalized using the typical values for the magnetosheath: d i = 10 km and ω ci = 0.6 Hz.
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Comparison of average values of −Π ij  D  ij /ρ and ﹩-\left({\boldsymbol{P}}\cdot {\rm{\nabla }}\right)\cdot {\boldsymbol{u}}/\rho ﹩ with the energy decay rates estimated at MHD scales for the collection of MMS intervals. Note that the factors of mass density ρ are used to convert energy per unit volume to energy per unit mass, the latter being the standard units used in incompressible turbulence theory. The computed rates have been accumulated into 11 bins and the average in each bin has been shown; positive values are represented using circles and negative values using diamond markers.